J/ApJ/950/89ivo://CDS.VizieR/J/ApJ/950/89doi:10.26093/cds/vizier/ba-xp-2sCDSLario D.Richardson I.G.Aran A.Wijsen N.2026-07-02T11:59:43Z2025-09-03T10:12:05ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frthe-sunsolar-systemgamma-ray-astronomyWe analyze periods with elevated >40MeV proton intensities observed near Earth over a time span of 43yr (1973-2016) that coincide with the passage of interplanetary (IP) shocks. Typically, elevated proton intensities result from large solar energetic particle (SEP) events. The IP shocks observed during these elevated-intensity periods may or may not be related to the origin of the SEP events. By choosing those cases when the shocks can be confidently associated with the solar eruption that generated the SEP event, we analyze the components of these SEP events that are localized in the vicinity of the shock (so-called "energetic storm particles", ESPs), focusing on those events where the ESP component exceeds 40MeV. We examine the interdependence of these high-energy ESPs with (i) the properties of the solar eruptions that generated the shocks and the SEP events, and (ii) the parameters of the shocks at their arrival at 1au. The solar eruptions at the origin of the shocks producing >40MeV proton ESP intensity enhancements are within +/-50{deg} longitude of central meridian and are associated with fast coronal mass ejections (plane-of-sky speeds >~1000km/s). The ESP events with the largest >40MeV proton intensity increases tend to occur when there are structures such as intervening IP coronal mass ejections and other unrelated shocks present in the solar wind through which the shock is propagating. Among the various local shock parameters considered, only the shock speed shows a certain degree of correlation with the observed ESP intensity increase.2023ApJ...950...89Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/950/89CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/440/373 : Earthbound interplanetary shocks (Howard+, 2005)J/ApJ/710/1111 : Observations of interplanetary shocks (Gopalswamy+, 2010)J/ApJ/903/125 : MHD simulations cases; Martian bow shock model (Wang+, 2020)J/A+A/640/A17 : CR Ground Level Enhancements spectra (IGLED) (Usoskin+, 2020)http://sepem.eu/ : ESA's Solar Energetic Particle Environment Modelling (SEPEM)http://ipshocks.helsinki.fi/database : Database of interplanetary shocks athttp://soho.nascom.nasa.gov/data/summary/solarwind/ : the CELIAS/MTOF Protonhttp://www.ssg.sr.unh.edu/mag/ace/ACElists/obs_list.html : ACE Lists ofhttp://lweb.cfa.harvard.edu/shocks/ : CfA Interplanetary Shock Databasehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/950/89https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/950/89http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/950/89https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/950/89https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/950/89http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/950/89GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-raydefaultJ/ApJ/950/89/table1*Selected shock passages occurring during enhanced ~40MeV proton intensitiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSolar cycle shock number (21-00 to 24-30)meta.id;meta.maincharprimaryTimeShock time; YYYY/DOY/hh:mm formattime.epochcharInstSpacecraft identifier (1)meta.id;instrcharParentParent Solar eruption time (2)time.epochcharf_ParentFlag on Parent (3)meta.codecharVT[474/2109]? Average transit speed of the shock to travel from the Sun to 1aukm/sphys.velocintnullableTheta[17/89]? Angle between upstream B field and shock normaldegpos.posAngintnullablee_Theta[0/39]? Uncertainty in Thetadegstat.error;pos.posAngintnullableVsc[278/1106]? Shock speed in spacecraft reference framekm/sphys.veloc;pos.frameintnullablee_Vsc[1/2357]? Uncertainty in Vsckm/sstat.error;phys.veloc;pos.frameintnullablef_VscFlag on Vsc (3)meta.codecharVsh[65/577]? Shock speed with respect to upstream solar windkm/sphys.veloc;arith.ratiointnullablee_Vsh[3/2358]? Uncertainty in Vshkm/sstat.error;phys.veloc;arith.ratiointnullablern[1.4/7.9]? Density compression ratiophys.density;arith.ratiofloatnullablee_rn[0.01/2.5]? Uncertainty in rnstat.error;phys.density;arith.ratiofloatnullableMms[0.4/6.2]? Magnetosonic Mach numberphys.veloc;arith.difffloatnullablee_Mms[0.03/1.3]? Uncertainty in Mmsstat.error;phys.veloc;arith.difffloatnullableMA[0.4/9.6]? Alfven Mach numberphys.veloc;arith.difffloatnullablee_MA[0.1/99]? Uncertainty in MAstat.error;phys.veloc;arith.difffloatnullablen_MAFlag on MA (4)meta.notecharJ/ApJ/950/89/table2Intensities measured during the passage of the shocks listed in Table 1IDSolar cycle shock number (21-00 to 24-30)meta.id;meta.maincharprimaryInc2